Simulating Ly Sources in the Epoch of Reionization AAR AARON SMI - PowerPoint PPT Presentation

Simulating Ly α Sources in the Epoch of Reionization AAR AARON SMI MITH Sakura Cosmic Lyman-Alpha Workshop Graduate Research Fellowship March 30, 2018 www.as.utexas.edu/~asmith Program

TALK OVERVIEW Si Sims Bi Big Ba Bang ng To Toda day Ob Obs Computer simulations connect what can be directly seen with what is ultimately powering celestial sources. We weave the snapshots accessible to observations into a continuous tapestry of cosmic evolution. ­ Frontiers in Lyman-alpha radiative transfer ­ Resonant Discrete Diffusion Monte Carlo (rDDMC) ­ Radiation hydrodynamics and zoom-in simulations

(SOME!) FRONTIERS IN MULTI-SCALE LYMAN-ALPHA RADIATIVE TRANSFER 10 0 Cosmic Ly α Transfer code (COLT) T = 1 K 10 - 1 T = 10 K x cw T = 500 K ­ Monte Carlo Methodology Empiri Em rical Mod odels L 10 - 2 T = 10 4 K (Sh (Shells/Clum umps) ­ Parallel: MPI + OpenMP approx H 10 - 3 Input: 10 - 4 Scattering MCRT 10 5 Probability 10 - 5 0 5 10 Hy Hybrid Methods x (Su Subgrid/Ap Approx) Simul Si ulation-bas based ed rDDMC hi high- z LA LAE sur urveys Ab Ab Initi tio Ap Approach (C (Cos osmol olog ogical e etc. Output: Flux vs. Frequency Ga Galaxy Simulations) Breaking Bre g the MC MCRT efficiency y barri rrier r with my y new re resonant DDMC MC method

RESONANT DISCRETE DIFFUSION MONTE CARLO (rDDMC) ✓ r J ◆ ✓ k ◆ ∂ J + ∂ ∂ J Discretized transfer equation leads 1 ∂ t = r · to a Monte Carlo interpretation. ∂ν ∂ν c 3 k 2 ' Skips scatterings if !mfp ≪ Δ' ) Diffusion in Space & Frequency ✱ Smith + (2017d)

APPLYING RADIATION HYDRODYNAMICS TO RESONANCE LINES On the fly 3D Ly α radiation hydrodynamics is feasible with • my new resonant discrete diffusion Monte Carlo method. Initial collapse of massive seed black holes, e.g. DCBHs. • Study line driven winds, e.g. massive stellar systems and • lanthanide-rich kilonova from binary neutron-star mergers. Scenarios where optically-thin approximations break down. •

LEVERAGING Ly α AND OTHER PROBES FOR NEW PERSPECTIVES Central starburst drives an outflow & the Ly α line is redshifted. IGM Monte Carlo Ly α Mo Ra Radiative Trans nsfer We need accurate Ly α RT simulations Ly Ly α ca can be used to o study fundamental that resolve both ph phys ysic ics, , source e pr proper perties ies, , lar arge-sc scale the ISM and IGM. envir en ironmen ments, an and ev even en dyn ynamic amics.

COSMOLOGICAL “ZOOM-IN” SIMULATION OF A REDSHIFT 5 GALAXY (GIZMO/FIRE, Ma et al. 2017) Ac Accurate tely ly m model th l the i ionizing r radiati tion to to o obta btain th the r recombi binati tion e emission. Fo Follow the resonant scattering in the ISM and d transmission through the IGM.

ROTATING CAMERA REVEALS NONTRIVIAL SIGHTLINE DEPENDENCE (CLOUDS, DOPPLER SHIFTS)

MORPHOLOGICAL DIFFERENCES IN THE LYMAN-ALPHA ENERGY DENSITY z z = 6.6 z z = 5

TIME-DEPENDENCE OF LYMAN-ALPHA PROPERTIES z z = 6.6 z z = 5

PROPERTIES OF THE EMERGENT Ly α LINE The Ly α line properties fluctuate in response to the star formation rate. Time- and sightline-weighted medians: M vir = 5x10 8 M ☉ , f esc,Ly α = 66%, T IGM = 40% Δ v peak = 130 km/s, FWHM = 172 km/s F LOS /F iso = 1 +/- 0.43, EW Ly α = 23 Ang

QUICK NOTE ABOUT KINEMATICS Even with strong feedback, the Ly α haloes are “blue” while the core is ”red”.

SUMMARY Ly α sources provide clues about • galaxy formation and evolution, CGM/IGM, large-scale structure, and the epoch of reionization. JWST/GMT/TMT/E-ELT will extend • our view into the high-z frontier. On the fly 3D Ly α RHD is feasible • with my new rDDMC method.